Optical and X-ray GRB Fundamental Planes as Cosmological Distance Indicators

Abstract

Gamma-Ray Bursts (GRBs), observed up to 𝑧 = 9.4, can be employed as standardized candles, extending the distance ladder beyond Supernovae Type Ia (SNe Ia, 𝑧 = 2.26). We standardize GRBs using the 3D fundamental plane relation among the rest-frame end time of the X-ray plateau emission, its corresponding luminosity, and the peak prompt luminosity. Combining SNe Ia and GRBs, we constrain the matter content Ω M = 0.299 ± 0.009 assuming a flat ΛCDM cosmology with and without correcting for selection biases and redshift evolution. Using a similar 3D correlation in optical, we find that our optical GRB sample is as efficacious in the determination of Ω M as the X-ray sample. We trimmed our GRB samples to achieve tighter planes to be used to simulate additional GRBs. We determined how many GRBs are needed to be used as standalone probes to achieve a comparable precision on Ω M to the one obtained by SNe Ia only. We achieve the error measurements derived using SNe Ia in (Conley et al. 2011) with 142 GRBs in optical considering the errorbars on the variables halved and in Betoule et al. (2014) with 284 optical GRBs, by considering that the error bars on the variables halved. Using a doubled sample (obtained by future machine learning approaches that allow both a lightcurve reconstruction and the estimates of GRBs for which the GRB is unknown) compared to our current one, with errorbars halved we will reach the same precision of (Scolnic et al. 2018) with 390 GRBs which will be uses as efficient standalone probes as SNe Ia by 2054.

Putting Flat $Λ$CDM In The (Redshift) Bin

“…We refer readers to the original texts for methodology. Objectively, QSOs constitute emerging cosmological probes [53,59] and are understandably less well developed than the SN and BAO; nevertheless, even now SN remain a work in progress [54]. In particular, there is considerable intrinsic scatter in the QSO data and there is an ongoing debate about the standardisability of the Risaliti-Lusso QSOs [56][57][58][59][60].…”

Consistency study of high- and low-accreting Mg ii quasars: No significant effect of the Fe ii to Mg ii flux ratio on the radius-luminosity relation dispersion

“…New alternate cosmological probes might help resolve this issue. Such probes include H starburst galaxy observations which reach to redshift 𝑧 ∼ 2.4 (Mania & Ratra 2012;Chávez et al 2014;González-Morán et al 2021;Cao et al 2020Cao et al , 2021aCao et al , 2022bJohnson et al 2022;Mehrabi et al 2022), quasar (QSO) angular size observations which reach to 𝑧 ∼ 2.7 (Cao et al 2017;Ryan et al 2019;Cao et al 2020Cao et al , 2021bZheng et al 2021;Lian et al 2021), QSO X-ray and UV flux observations which reach to 𝑧 ∼ 7.5 (Risaliti & Lusso 2015Khadka & Ratra 2020a,b, 2021Lusso et al 2020;Rezaei et al 2022;Luongo et al 2021;Dainotti et al 2022a), 1 and gammaray burst observations that reach to 𝑧 ∼ 8.2 (Wang et al 2016(Wang et al , 2022Fana Dirirsa et al 2019;Demianski et al 2021;Khadka & Ratra 2020c;Khadka et al 2021c;Hu et al 2021;Luongo & Muccino 2021;Cao et al 2022c,d,a;Dainotti et al 2022b).…”

Gamma-ray burst data strongly favor the three-parameter fundamental plane (Dainotti) correlation relation over the two-parameter one

“…These results show that for both GRB samples the correlation slope a remains consistent within less than 2σ with the value of the correlation slope corrected for selection biases and evolutionary effects (Dainotti et al 2013), highlighting that the physics behind the correlation, namely that the energy reservoir remains constant, is consistently maintained, independent of the sample and cosmology used. (Note that here we do not use the correction for selection biases as used in Dainotti et al 2022b). Also, the positive correlation between the peak prompt luminosity and the luminosity at the end of the plateau emission, the L peak − LX correlation, is maintained at the 2σ level when compared with the intrinsic correlation corrected for selection biases which yield b = 1.14 +0.42 −0.16 (Dainotti et al 2015a).…”

“…Given the current paucity of GRB data it is therefore necessary to increase the sample size to allow the 3D correlation to have cosmological constraints comparable to those from SNIa data. A detailed study on simulating GRB constraints based on the Platinum sample to determine the number of Platinum-quality GRBs needed to reach constraints similar to those from a number of recent SNIa data sets is presented in Dainotti et al (2022b). To achieve similar GRB constraints one needs to wait for more GRB data from future missions, and one can use machine learning techniques and lightcurves reconstruction on these larger data sets that can enable smaller scatter (47.5%) on the 2D and 3D relation parameters.…”